Explosion of white dwarfs

Details Explosion of white dwarfs Explosion of white dwarfs

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.131..413l&link_type=abstract

(IAU, Colloquium on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, 93rd, Bamberg, West

Astronomy and Astrophysics

Astrophysics

Binary Stars, Light Curve, Nuclear Fusion, Stellar Evolution, Supernovae, White Dwarf Stars, Nickel Isotopes, Spectral Energy Distribution, Stellar Mass Ejection, Stellar Models, Supernova Remnants

Scientific paper

Models for Type I supernova light curves are presented which are based on the assumption of the explosion of partially solid white dwarfs in close binary systems leaving bound remnants of different sizes. The model constrains the mass of these remnants to less than 0.4 solar masses, and it reproduces quite well the maximum luminosities, the expansion velocities, and the shape of the light curve. Variations of the two basic parameters governing the light curve, the ejected mass and the mass of Ni-56 produced, reproduce the slow and fast subclasses of classical Type I supernovae. The synthesized quantity of Ni-56 is shown to lie between 0.6 and 1.0 solar mass.

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